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A Few Tens au Scale Physical and Chemical Structures Around Young Low-Mass ProtostarsIRAS 15398–3359

A Few Tens au Scale Physical and Chemical Structures Around Young Low-Mass Protostars: IRAS... [Sub-arcsecond (0.″5\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$0{.\!\!^{\prime \prime }}5$$\end{document}; 80 au) images of the H2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$_2$$\end{document}CO and CCH lines have been obtained toward the low-mass protostellar source IRAS 15398−3359 in the Lupus 1 cloud with Atacama Large Millimeter/Submillimeter Array. A compact component concentrated in the vicinity of the protostar has been detected as well as a well-collimated outflow cavity extending along the northeast-southwest axis. The inclination angle of the outflow is found to be about 70∘\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$70{^\circ }$$\end{document} based on the observed kinematic structure. This nearly edge-on configuration is in contrast to previous suggestions of a pole-on geometry. The centrally concentrated component is interpreted with the aid of an infalling-rotating envelope model employing the inclination angle obtained from the outflow structure, and the protostellar mass is estimated to be less than 0.09M⊙\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$0.09\ M_\odot $$\end{document}. A rotationally-supported disk in this source is hinted at by a weak high-velocity H2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$_2$$\end{document}CO emission associated with the protostar, to confirm whose presence higher-spatial resolution observations are needed.] http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png

A Few Tens au Scale Physical and Chemical Structures Around Young Low-Mass ProtostarsIRAS 15398–3359

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Publisher
Springer Nature Singapore
Copyright
© Springer Nature Singapore Pte Ltd. 2022
ISBN
978-981-19-1707-3
Pages
71 –87
DOI
10.1007/978-981-19-1708-0_5
Publisher site
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Abstract

[Sub-arcsecond (0.″5\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$0{.\!\!^{\prime \prime }}5$$\end{document}; 80 au) images of the H2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$_2$$\end{document}CO and CCH lines have been obtained toward the low-mass protostellar source IRAS 15398−3359 in the Lupus 1 cloud with Atacama Large Millimeter/Submillimeter Array. A compact component concentrated in the vicinity of the protostar has been detected as well as a well-collimated outflow cavity extending along the northeast-southwest axis. The inclination angle of the outflow is found to be about 70∘\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$70{^\circ }$$\end{document} based on the observed kinematic structure. This nearly edge-on configuration is in contrast to previous suggestions of a pole-on geometry. The centrally concentrated component is interpreted with the aid of an infalling-rotating envelope model employing the inclination angle obtained from the outflow structure, and the protostellar mass is estimated to be less than 0.09M⊙\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$0.09\ M_\odot $$\end{document}. A rotationally-supported disk in this source is hinted at by a weak high-velocity H2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$_2$$\end{document}CO emission associated with the protostar, to confirm whose presence higher-spatial resolution observations are needed.]

Published: Nov 9, 2022

Keywords: Low-mass protostar; Protostellar disks; Jets and outflows; Interstellar medium; Individual (IRAS 15398−3359)

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